frontier science with the james webb space telescope › science-red › s3fs... · instrumentation...

Frontier Science with the James Webb Space Telescope

Jason Kalirai (STScI)

Oct 20th, 2011 Astrophysics Subcommittee Meeting, NASA HQ

Frontier Science with JWST

Outline1.) Two Slide Primer2.) Instrumentation3.) Frontier Science

- Solar System- Exoplanets- Resolved Stellar Pops in the Milky Way - Resolved Stellar Pops in the Local Volume- First Galaxies and Stars- Dark Energy

4.) Community Tools

100 microns10 microns1 micronsWavelength

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HST

Spitzer

JWST

1.) Photon Limited Science2.) Diffraction Limited Science

JWST is Astronomy’s Next Great Observatory

1.) Photon Limited Science2.) Diffraction Limited Science

Hubble (D = 2.4 m)ACS @ 0.5 mm = 0.043’’WFC3 @ 1.6 mm = 0.138’’

Spitzer (D = 0.8 m)IRAC @ 3.6 mm = 0.93”IRAC @ 8.0 mm = 2.06”MIPS @ 24 mm = 6.18”

JWST (D = 6.5 m)NIRCam @ 2 mm = 0.063’’NIRCam @ 4 mm = 0.126’’MIRI @ 10 mm = 0.317’’MIRI @ 20 mm = 0.635’’

Diffraction Limits

But, Hubble pixels are 0.04 – 0.05” at <1 mm and 0.13” at >1 mmSpitzer pixels are 1.2” at <8 mm and 2.55” at 24 mm

Hubble can not achieve Nyquist sampling of the diffraction limitSpitzer only achieves Nyquist sampling of limit at l > 24 microns

JWST NIRCam has two modules, with pixel size 0.0317” at <2.5 mm and 0.0648 at >2.5 mmJWST MIRI has pixel size of 0.11 arcsec

JWST achieves Nyquist sampling of the diffraction limit at 2 mm, 4 mm, and 7+ mm

JWST is Astronomy’s Next Great Observatory

The Hubble UDF(F105W, F125W, F160W)

Simulated JWST

The Near Infrared Camera (NIRCam)- Visible and near infrared camera (0.6 – 5 micron)- 2.2’ x 4.4’ field of view, diffraction limited- Coronographs

The Near Infrared Spectrograph (NIRSpec)- Multi-object spectrograph (1 – 5 micron)- 3.4’ x 3.4’ FOV, 0.1” pixels- R = 1000 and 2700 gratings; R = 100 prism- 3” x 3” IFU

NIRCam

NIRSpec

JWST Instruments: Imaging, Spectroscopy, & Coronography

The Mid Infrared Instrument (MIRI)- Mid-infrared camera and spectrograph (5 – 28 microns)- 1.9’ x 1.4’ imaging FOV, 0.11” pixels- R = 100 slit spectrograph (5 – 10 micron) and IFU (R = 3000)- Coronographs

The Near Infrared Imager and Slitless Spectrograph (NIRISS)- Infrared imager and slitless spectrograph- 2.2’ x 2.2’ FOV

The Fine Guidance Sensor (FGS)- 2.4’ x 2.4’ imager for target acquisition- Rapid readout of subarray for ACS control- 95% probability of finding a guide star anywhere in sky

MIRI

NIRISS and FGS

JWST Instruments: Imaging, Spectroscopy, & Coronography

Program- Nearly 200 participants- Mix of invited and contributed talks focusing on science potential- 40 poster presentations- 1/3 of total time was reserved for discussion- PIs described instrument capabilities to deliver forefront science- Public Talk, Education Display, Hubble 3D viewing, Science Writers Workshop, …

SOC Chair – Wendy Freedman STScI – June 6 – 8th, 2011

Frontier Science Opportunities with JWST

Science Highlights

•Strong Lensing to Study the Evolution of Galaxies – Tommaso Treu (UCSB)

•High Precision Measurements of H0 – Adam Riess (STScI / JHU)

•Finding the First Cosmic Explosions with JWST – Daniel Whalen (Carnegie Mellon Univ.)

•A Compendium of Kepler Discoveries for JWST Follow Up – William Borucki (NASA ARC)

•Observing the First Galaxies – Richard Ellis (Caltech)

•Solar System Opportunities with JWST – Heidi Hammel (AURA)

•Gas in Protoplanetary Disks – Thomas Henning (MPIA)

•Active Galactic Nuclei with JWST – Jane Rigby (GSFC)

•Star Formation in Galaxies in the Era of JWST – Daniela Calzetti (UMass)

•Mid Infrared Observations of High Redshift Galaxy Evolution – Alexandra Pope (UMass)

https://webcast.stsci.edu/webcast/(Click “Webcast Archives”)


https://webcast.stsci.edu/webcast/

Science Highlights

•Exotic Endings for Massive Stars – Shri Kulkarni (Caltech)

•Robust Predictions for High-z Galaxies: What will we Learn with JWST – Andrew Benson (Caltech)

•The “Final Frontier” of Star & Planet Formation:Piled Deeper & Wider – Mike Meyer (ETH,Zurich)

•Exoplanet Discovery and Characterization with JWST – Jeff Valenti (STScI)

•Weaving Circumgalactic Webs: The View from the Webb Telescope – Crystal Martin (UCSB)

•The Evolution of Chemical Enrichment and Outflows at z ~ 1-6 – Alice Shapley (UCLA)

•Probing Galaxy Stellar Mass Assembly in the Universe with JWST – Karina Caputi (Edinburgh)

•Resolved Stellar Populations in the Near IR – Jason Kalirai (STScI)

•Probing the Dissipation of K.E. In Phases of Galaxy Evol. with JWST – Pierre Guillard (Caltech)

•Star Formation in the Milky Way and its Neighbors in the Mid-IR – Christine Wilson (McMaster)




Solar System Science with JWST

"There are three main areas in which collaboration with other parts of NASA could benefit the solar system exploration program....the Hubble Space Telescope has a long history of successful planetary observations, and this collaboration can be a model for future telescopes such as the James Webb Space Telescope.”

Hubble, Spitzer, and Herschel

- Discovery of new moons around Pluto

- Discovery of the largest ring around Saturn

- Characterization of Ceres and Vesta, others

- Discovery of new Kuiper Belt Objects (KBOs)

- Detailed studies of cloud structure in Gas Giants

- Torus of water vapor on Saturn

- Ocean-like water on Jupiter-family comet

- Long-term monitoring of the Martian atmosphere

- And much more…

Vision and Voyages for Planetary Science in the Decade 2013-2022

Pointing Control System

Enables observations of solar system objects with rates of motion up to 0.03 arcsec per second. Includes all planets and asteroids beyond Earth’s orbit.

Mars

• Time-resolved NIR spectroscopy will reveal the variability of atmospheric species including

CO2, CO, and H2O and constrain radiative and absorptive properties of airborn dust,

enabling photochemical and dynamical modeling of the Martian climate.

Jupiter and Saturn

• MIR med-res. spectroscopy and IFU data will explore phosphine and methane fluorescence,

which link to the vertical dynamics and thermal structure of the upper atmosphere.

• Provide a global context on large-scale weather patterns for high-resolution studies from

complementary planetary missions (e.g., Juno and Cassini).


Uranus and Neptune

• Image spectral features from high latitudes in each planet with high sensitivity and map clouds.

• Spectral characterization of H3+, CO in fluorescence, detailed mapping of 5 micron window,

search for minor species, and measure isotopic ratios of major elements.

• MIR observations will measure temporal variations in temperature, resolve sources of

underlying driving dynamics, and disentangle causes of rotation modulation.


Pointing Control System

Enables observations of solar system objects with rates of motion up to 0.03 arcsec per second. Includes all planets and asteroids beyond Earth’s orbit.

Mars

• Time-resolved NIR spectroscopy will reveal the variability of atmospheric species including

CO2, CO, and H2O and constrain radiative and absorptive properties of airborn dust,

enabling photochemical and dynamical modeling of the Martian climate.

Jupiter and Saturn

• MIR med-res. spectroscopy and IFU data will explore phosphine and methane fluorescence,

which link to the vertical dynamics and thermal structure of the upper atmosphere.

• Provide a global context on large-scale weather patterns for high-resolution studies from

complementary planetary missions (e.g., Juno and Cassini).

Kuiper Belt Objects (KBOs)

•Image all known KBOs in the MIR

•R = 100 NIR spectroscopy with S/N = 20 in 3 hours (V < 25); R>100 for bright KBOs

1.) Constrain surface compos. (H2O,CH4,CH3OH) & volatile inventories; first spectra at 2.5–5 microns.

2.) Address the dynamical and chemical history of the solar system; test formation theories.

Artist’s impression of a binary KBO


Dwarf Planets

•Time-resolved imaging of Pluto, Eris, Sedna and other dwarf planets

•IR spectroscopy of large bodies in the outer solar system

1.) Reveal seasonal behaviors and surface compositions.

2.) Track variations in N2 and CH4; discover new organic molecules/ices.

3.) Explore correlations between atmospheric chemistry changes and albedo.

The Mass of Eris

(Hubble + Keck)







…and much more, including Icy Moons and Comets

1.) Lunine, J. et al. (2010), “JWST Planetary Observations within the Solar System”

2.) Sonneborn, G. et al. (2009), “JWST Study of Planetary Systems and Solar System Observations”

3.) Planetary Science with JWST Flyer, http://www.stsci.edu/jwst/news/2011/DPS2011_JWSTFlyer.pdf


Dwarf Planets

•Time-resolved imaging of Pluto, Eris, Sedna and other dwarf planets

•IR spectroscopy of large bodies in the outer solar system

1.) Reveal seasonal behaviors and surface compositions.

2.) Track variations in N2 and CH4; discover new organic molecules/ices.

3.) Explore correlations between atmospheric chemistry changes and albedo.






http://www.stsci.edu/jwst/doc-archive/white-papers/JWST_Solar_System.pdf



http://www.stsci.edu/jwst/doc-archive/white-papers/JWST_planetary.pdf



http://www.stsci.edu/jwst/news/2011/DPS2011_JWSTFlyer.pdf

Exoplanet Discovery and Characterization with JWST

Kepler

Planetary candidates in 1st data release

• 1235 candidates

• 68 Earth-sized planets

• 54 candidates in habitable zone

• 5.4% of stars host Earth sized planetary candidate

Transiting Exoplanet Survey Satellite (TESS)

• Selected NASA Explorer Proposal for Potential Future Mission

Application Planet Type Res. JWST Scientific Investigations

Transit Light Curves Gas GiantsIntermediate MassSuper EarthsTerrestrial Planets

5555

- Planet prop. w/ RVs (mass, radius) physical structure- Detection of terrestrial transits- Transit timing: detection of unseen planets

Phase Light Curves Gas GiantsHot Neptunes

55

- Day to night emission mapping- Dynamical models of atmospheres

Transmission Spectroscopy

Gas GiantsIntermediate MassSuper Earths

3000100-500<100

- Spectral line diagnostics- Atmospheric composition measurements (C, CO2, CH4)- Follow up of survey detections

Emission Spectroscopy

Gas GiantsIntermediate MassSuper Earths

3000100-500<100

- Spectral line diagnostics- Temperature measurements- Follow up survey detections

M. Clampin et al. (2009), JWST White Paper, “Comparative Planetology: Transiting Exoplanet Science with JWST”

JWST/NIRSpec will measure phase curves of exoplanets around nearbyM dwarfs in 1 hour.


Atmospheric transmission spectrum (4 hours) for HD209458-like Kepler source using NIRSpec (R=3000). Simulation from J. Valenti

JWST can detect water in habitable zone Super Earths.


Local Calibrators

• Star clusters represent excellent tools for testing stellar evolution models

• Constituent stars are coeval, iso-metallic, and co-spatial

• HST has been a game changer, especially at visible wavelengths

JWST and Resolved Stellar Pops in the Milky Way

Complete Stellar Pops of a ClusterJ. Kalirai et al. (2011, submitted)

A wide-field view of 47 Tuc and the SMC

Local Calibrators

• JWST will be a game changer with IR high resolution, wide field capability

The predicted color-magnitude diagram shape for a coeval population at 10 kpc

- “Kink” is age insensitive, removes degeneracies

- Accurate fundamental parameters

- New tests of stellar evolution models in the IR

- New generations of pop. synthesis models

- Measure total stellar pop more efficiently


J. Kalirai et al. (2011, submitted)

First hints from WFC3/IR

JWST will measure V = 30 M dwarfs in 10 minutes.

JWST will measure the stellar mass function to the H burning limit in stellar

populations out to 25 kpc in <3 hours.


• NIRSpec will obtain large (~104) statistical samples of spectra in dense fields, 10-40% recovery.

• MSA reconfiguration once, no dithering. Sky background exposures are “free”.

• Use cases in globular clusters, star forming regions, Galactic disk, Galactic bulge, provided user requires statistical sampling of stars.

+ Targets in operable shutter x Targets outside shutters

Combine JWST photometry with JWST spectroscopy

A Simulated Field of Omega Cen and the NIRSpec Microshutter Array (MSA)


Combine JWST photometry with JWST spectroscopy

Putting it Together• NIRCam, NIRISS imaging & NIRSpec MOS spectroscopy of clusters, MW components, and star

forming regions will provide age & abundances and test formation & assembly models.

• NIR imaging completes stellar inventory of MW pops and informs the Galactic mass budget.

• MIRI imaging & spectroscopy provides Teff, log(g), and mass for stellar and substellar objects.


+ Targets in operable shutter x Targets outside shutters

A Simulated Field of Omega Cen and the NIRSpec Microshutter Array (MSA)

Synergy between wide-field ground based imaging, HST ultra-deep imaging and and 10-m spectroscopy

SDSS Field of Streams

Brown et al. (2008)

SDSS, HST, & Keck work together to yield substructure maps,

metallicity, ages, and kinematics of nearby Local Group galaxies.

JWST and Resolved Stellar Pops in the Local Volume

Future synergies between LSST, JWST, and 30-m telescopes will 1.) Push beyond the Local Group2.) Increase leverage to probe sensitive age variations.

T. Brown et al. (2008), JWST White Paper,”Studying Resolved Stellar Populations with JWST”

JWST will yield the first direct ages in galaxies outside the Local Group in 10 hours.

Extended SFH will be efficiently measured with filters well-separated in wavelength

and with larger FOVs than Hubble.

JWST and Resolved Stellar Pops in the Local Volume

http://www.stsci.edu/jwst/doc-archive/white-papers/stellarPops_v4d.pdf



JWST will Study the First Galaxies

Why measure galaxies in the Universe’s first billion years?

•Seeds of today’s galaxies started growing.

•Dark matter halos of massive galaxies first formed.

•Significant metals first formed.

•When the Universe was reionized.

JWST will resolve ambiguities from Hubble and Spitzer in fitting SEDs by spectroscopically

characterizing early systems at z = 9, and characterizing stellar contributions to z > 10.

JWST and First Galaxies

A candidate z ~ 10 galaxy; Bouwens et al. (2011)

The Star Formation Rate Density vs Redshift; Oesch et al. (2011)

Hints from Hubble that a big change is occurring 400 – 600 Myr after the Big Bang.

JWST will provide a robust picture of the number of galaxies and their properties.

May need help from gravitational lensing (do homework now).

How do we know if we’ve found the first galaxies? See R. Ellis’ talk on Frontiers webcast.


JWST and 30-m Telescopes Synergy

http://www.tmt.org/science-case

“The nature of “first-light” objects and their effects on the young universe areamong the outstanding open questions in astrophysics. Here TMT and the JamesWebb Space Telescope (JWST) will work hand-in-hand, with JWST providing thetargets for detailed study with TMT’s spectrometers.”


Properties•Thought to be very massive (25 – 500 Msun)•Form in isolation•Tsurface ~ 100,000 K•Luminous sources of ionizing photons (> 1050 /s)•2-3 Myr lifetimes

D. Whalen – Frontiers Talk

New simulated light curves show late time rise over > 100 days.

Infrared energy diffuses out through dense ejecta of PI SNe…

can be measured with JWST to z > 10 and maybe 15 with strong lensing in this model.

Ground based follow up with 30-m telescopes will help distinguish progenitors.

JWST and First Supernovae

A. Riess’ Talk at Frontiers Meeting1.) JWST is the only telescope that can measure type Ia SNe out to z = 3.5

2.) JWST will characterize Cepheids in further galaxies•Calibrate more type Ia SNe•Simpler in the IR, less scatter

3.) H0 to 1%, ties down ties local expansion rate.

4.) Planck CMB gives distance scale at z = 1000.

Two measurements provide an over constrained problem. Take one of the measurements, vary the cosmological model (i.e., w) to match the other.

JWST and Dark Energy



JWST and Other Science from the Frontiers Science Meeting

•Gas in Protoplanetary Disks – Thomas Henning (MPIA)

•Star Formation in Galaxies in the Era of JWST – Daniela Calzetti (UMass)

•Exotic Endings for Massive Stars – Shri Kulkarni (Caltech)

•The “Final Frontier” of Star and Planet Formation: Piled Deeper and Wider – Mike Meyer (ETH Zurich)

•Star Formation in the Milky Way and its Neighbors in the Mid-IR – Christine Wilson (McMaster)

•Strong Lensing to Study the Evolution of Galaxies – Tommaso Treu (UCSB)

•Active Galactic Nuclei with JWST – Jane Rigby (GSFC)

•Mid Infrared Observations of High Redshift Galaxy Evolution – Alexandra Pope (UMass)

•Weaving Circumgalactic Webs: The View from the Webb Telescope – Crystal Martin (UCSB)

•The Evolution of Chemical Enrichment and Outflows at z ~ 1-6 – Alice Shapley (UCLA)

•Probing Galaxy Stellar Mass Assembly in the Early Universe with JWST – Karina Caputi (Edinburgh)

•Probing the Dissipation of K.E. In Phases of Galaxy Evolution with JWST – Pierre Guillard (Caltech)


Scientific Discovery Potential

Find the First Stars and Galaxies

Map the Evolution of Galaxies

Unveil Newborn Solar Systems

Find Water on Other Planets

Dark Energy and the Universe’s Expansion

Gravitational Lensing and Dark Matter

The Age of The Universe

Supermassive Black Holes

Imaging and Spectroscopy of Exoplanets

???

Science GoalsScience Discoveries

The Extragalactic Distance Scale and Hubble Constant

Origin and evolution of Solar System

Gas in Galaxies and Quasar Absorption Lines

Intensities of Supernovae

Ages of Stellar Pops Beyond Milky Way

Source of Gamma Ray Bursts

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JWST Exposure Time Calculator – http://jwstetc.stsci.edu/etc/JWST PSF Tool – http://www.stsci.edu/jwst/software/webbpsf.htmlJWST Email For Community Input – [email protected] Facebook Page For Astronomers – “JWST Observer”JWST Twitter – @auraJWST

http://jwstetc.stsci.edu/etc/

http://www.stsci.edu/jwst/software/webbpsf.html

mailto:[email protected]

JWST Exposure Time Calculator – http://jwstetc.stsci.edu/etc/JWST PSF Tool – http://www.stsci.edu/jwst/software/webbpsf.htmlJWST Email For Community Input – [email protected] Facebook Page For Astronomers – “JWST Observer”JWST Twitter – @auraJWST


http://jwstetc.stsci.edu/etc/

http://www.stsci.edu/jwst/software/webbpsf.html

mailto:[email protected]

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